J/ApJ/701/587 A deep HST H-band imaging survey. II. QUEST QSOs (Veilleux+, 2009)
A deep Hubble space telescope H-band imaging survey of massive gas-rich mergers.
II. The QUEST QSOs.
Veilleux S., Kim D.-C., Rupke D.S.N., Peng C.Y., Tacconi L.J., Genzel R.,
Lutz D., Sturm E., Contursi A., Schweitzer M., Dasyra K.M., Ho L.C.,
Sanders D.B., Burkert A.
<Astrophys. J., 701, 587-606 (2009)>
=2009ApJ...701..587V 2009ApJ...701..587V
ADC_Keywords: Galaxies, IR ; Magnitudes, absolute ; Morphology ; Surveys ; QSOs
Keywords: galaxies: active - galaxies: interactions - galaxies: Seyfert -
galaxies: starburst - infrared: galaxies
Abstract:
We report the results from a deep Hubble Space Telescope (HST) NICMOS
H-band imaging survey of 28 z<0.3 QSOs from the Palomar-Green (PG)
sample. This program is part of QUEST (Quasar/ULIRG Evolution Study)
and complements a similar set of data on 26 highly nucleated ULIRGs
presented in Paper I (Veilleux et al. 2006ApJ...643..707V 2006ApJ...643..707V). Our
analysis indicates that the fraction of QSOs with elliptical hosts is
higher among QSOs with undetected far-infrared (FIR) emission, small
infrared excess (LIR/LB<10), and luminous hosts. The hosts of
FIR-faint QSOs show a tendency to have less pronounced merger-induced
morphological anomalies and larger QSO-to-host luminosity ratios on
average than the hosts of FIR-bright QSOs, consistent with late-merger
evolution from FIR-bright to FIR-faint QSOs.
Description:
The methods used to acquire, reduce, and analyze the present data are
nearly identical to those of Paper I (Veilleux et al. 2006ApJ...643..707V 2006ApJ...643..707V)
in which we reported the results from a Cycle-12 HST NICMOS H-band
imaging survey of 26 z<0.3 ULIRGs and seven infrared-bright
Palomar-Green (PG) QSOs. The combined sample of 28 PG QSOs
successfully observed during Cycles 12 and 15 covers the low-redshift
and low B-band luminosity ends of the PG QSO sample (see Figure 2 of
Veilleux et al. 2009, Cat. J/ApJS/182/628).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 82 28 PG QSOs sample
table5.dat 85 28 *Summary results from the GALFIT analysis
table6.dat 61 217 Black Hole Mass
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Note on table5.dat : Entries in this table are the parameters from the
best-fitting one- or two-galaxy component models (tables 2 and 3 of the paper).
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See also:
VIII/13 : A new catalog of 53522 4.85GHz sources (Becker+ 1991)
J/ApJS/182/628 : Spitzer quasar and ULIRG evolution study (Veilleux+, 2009)
J/ApJ/666/806 : SED of Spitzer quasars (QUEST) (Netzer+, 2007)
J/AJ/131/1923 : Known quasars in the QUEST Variability Survey (Rengstorf+,
2006)
J/ApJ/613/682 : AGN central masses and broad-line region sizes (Peterson+,
2004)
J/ApJS/143/315 : IRAS 1Jy sample of ultraluminous galaxies. II. (Veilleux+,
2002)
J/AJ/108/1163 : Radio structure of Quasars (Kellermann+ 1994)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Object name
13- 22 A10 --- OName Other name
24- 28 F5.3 --- z Redshift
30- 35 F6.2 [Lsun] logLB Blue luminosity
37 A1 --- l_logLIR Limit flag on logLIR
38- 42 F5.2 [Lsun] logLIR ? Infrared luminosity (1)
44- 48 F5.2 [Lsun] logLbol Bolometric luminosity (2)
50 A1 --- l_LIR/LB Limit flag on LIR/LB
51- 55 F5.2 --- LIR/LB ? Ratio of infrared to blue luminosities
57 A1 --- l_LIR/Lbol Limit flag on LIR/Lbol
58- 61 F4.2 --- LIR/Lbol ? Ratio of infrared to bolometric luminosities
63 A1 --- l_F25/F60 Limit flag on F25/F60
64- 68 F5.3 --- F25/F60 25/60µm flux ratio
69 A1 --- u_F25/F60 [:] Uncertainty flag on F25/F60
71 A1 --- RL [LQ] Radio loudness (Q=quiet vs L=loud) (3)
73- 82 A10 --- Class FIR strength: Strong, Weak or Undetected (4)
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Note (1): Infrared luminosity calculated from prescription of
Sanders & Mirabel (1996ARA&A..34..749S 1996ARA&A..34..749S).
Note (2): Bolometric luminosity calculated from 7xL(5100Å)+L(IR)
(Netzer et al. 2007, Cat. J/ApJ/666/806)
Note (3): From Kellermann et al. (1994, Cat. J/AJ/108/1163) except for two
objects (B2 2201+31A and PG2349-014 from Becker et al. 1991, Cat. VIII/13).
Note (4): far-IR strength according to Netzer et al. (2007, Cat. J/ApJ/666/806)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Object name
12 A1 --- u_Name [b] uncertain values (1)
14- 19 F6.2 mag MAGt Total absolute magnitude (host+PSF-comp.)
21- 26 F6.2 mag MAGp Absolute magnitude of PSF component
28- 33 F6.2 mag MAGh Absolute magnitude of host galaxy (including
tidal features)
35- 40 F6.2 mag MAGm Absolute magnitude of best-fitting galaxy
host model
42- 46 F5.2 --- Ip/Ih PSF-to-host intensity ratio
48- 51 F4.2 --- Im/Ih Model-to-host intensity ratio
53- 56 F4.2 kpc r1/2 ? Half-light radius of n=4 Sersic component
58- 62 F5.2 mag/arcsec2 <mu1/2> ? Mean surface brightness of n=4 Sersic
component within half-light radius
in Hmag/arcsec2
64- 67 A4 --- Bar [Yes?/No ] Presence of a stellar bar?
69- 72 A4 --- Arms [Yes?/No ] Presence of spiral arms?
74- 77 A4 --- Dis [Yes?/No/Str ] Presence of merger-induced
disturbance (Str=strongly disturbed)
79- 81 A3 --- MType Morphological class (2)
83- 85 A3 --- IC Interaction class (IVb or V) (3)
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Note (1): Entries for this object are uncertain because the host galaxy
fills most of the field of view, so the sky background is not well
determined.
Note (2): Morphological classes are:
E = elliptical,
B+D = bulge+disk,
D = disk,
A = ambiguous.
Question marks ("?") indicate uncertain classification
due to PSF mismatch (see sections 3 and 4.1).
Note (3): IVb = compact merger, V = old merger; see Veilleux et al. 2002,
Cat. J/ApJS/143/315, section 3.4, for details on the definitions.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Sample [ULIRGs/PG QSOs]
9- 24 A16 --- Name Galaxy name
26- 32 F7.2 10+7Msun Mph ? Black hole mass from spheroid luminosity
34- 39 F6.3 10+7Msun Mdyn ? Black hole mass from spheroid velocity
dispersion
41- 46 F6.2 10+7Msun Mrev ? Black hole mass from reverberation mapping
48- 53 F6.2 10+7Msun Mvir ? Black hole mass from virial relation
55- 61 A7 --- Ref MBH reference(s) (1)
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Note (1): References as follows:
1 = Dasyra et al. 2006ApJ...651..835D 2006ApJ...651..835D
2 = Veilleux et al. 2002, Cat. J/ApJS/143/315
3 = Veilleux et al. 2006ApJ...643..707V 2006ApJ...643..707V
4 = Dasyra et al. 2006ApJ...638..745D 2006ApJ...638..745D
5 = This paper;
6 = Peterson et al. 2004, Cat. J/ApJ/613/682
7 = Dasyra et al. 2007ApJ...657..102D 2007ApJ...657..102D
8 = Vestergaard & Peterson 2006ApJ...641..689V 2006ApJ...641..689V
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History:
From electronic version of the journal
References:
Veilleux et al. Paper I. 2006ApJ...643..707V 2006ApJ...643..707V
(End) Emmanuelle Perret [CDS] 12-Sep-2011